NASA Planetary Science Division s Instrument Development Programs, PICASSO and MatISSE

Transcription

1 NASA Planetary Science Division s Instrument Development Programs, PICASSO and MatISSE James R. Gaier NASA Planetary Science Division

2 NASA Planetary Science Strategic Objective: Ascertain the content, origin, and evolution of the solar system and the potential for life elsewhere. It seeks to address this objective with five fundamental goals: Explore and observe the objects in the solar system to understand how they formed and evolve. Advance the understanding of how the chemical and physical processes in our solar system operate, interact, and evolve. Explore and find locations where life could have existed or could exist today. Improve our understanding of the origin and evolution of life on Earth to guide our search for life elsewhere. Identify and characterize objects in the solar system that pose threats to Earth or offer resources for human exploration. 2

3 Instrument Development Strategy PICASSO MatISSE Flight Instrument I have this crazy idea TRL 1-3 I can make it work TRL 4-6 How did we ever do without it? TRL

4 Planetary Instrument Concepts Advancing Solar System Observations (PICASSO) PICASSO supports the development of spacecraft-based instrument systems that show promise for use in future planetary missions Program goal to develop low TRL technology to feed MatISSE, etc. science instrument feasibility studies concept formation proof of concept instruments advanced component technology Program objectives to develop new technologies that significantly improve instrument measurement capabilities for planetary science missions Proposals are typically sought every year. The budget is ~$3.5 M per year. Average award ~ $250 - $300K/year Typically 12 awards 4

5 Maturation of Instruments for Solar System Exploration (MatISSE) MatISSE supports the maturation of spacecraft-based instrument systems that show promise for use in future planetary missions Program goal to develop instrument to point where they can be proposed to flight programs Must address specific science objectives Retire major technological risk Program requires higher level of oversight Quarterly reviews Site visits External reviewers Proposals are typically sought on even numbered years The budget is ~$6 M per year. Average award ~ $1.0M/year Typically 6 awards 5

6 Instruments Being Developed for Venus Planetary Heat-Flux Sensor for Venus Michael Pauken JPL Glass-based pressure seal Ni alloy wires in fiberglass sleeves High Temperature Electronics Gary Hunter NASA GRC Before Venus test 3mm x 3mm SiC Chip Ceramic substrate After Venus test Airborne Electromagnetic Sounding of the Interiors of Venus, Mars, and Titan Bob Grimm SWRI Piezoelectric Micro Valve for Atmospheric Descent Sampling Jurij Simcic JPL 6

7 TRL 6 Instruments Adapted Development of an Instrument to Measure Turbulent Eddy Fluxes in Planetary Atmospheres (Scott Rafkin/SWRI) Europa Short Wavelength InfraRed Spectrometer - Radiation and Planetary protection Maturation ESWIRS-RPM (Bob Green.JPL) CIRIS: A near- and mid-infrared Fourier transform spectrometer for investigations of the surface composition and habitability of Europa. (Kevin Hand/JPL) SIRSE: Spectral ImageR/ Spectrometer for Europa (Dennis Reuter/GSFC) Adapting and testing micro mass spectrometers to identify biomarkers for astrobiology missions (Frisco van Ameron) Technical development of the MASPEX instrument for Europa Exploration (Jack Waite/SWRI) A Probe For Europa's Plasma Interaction (Frances Bagenal/Colorado) Development of Large Format Rad-Hard Focal Plane Arrays and Readouts for Thermal Radiometer for Europa Clipper Mission (Matt Kenyon/JPL) Planetary Instrument for Submillimeter-wave Surface and Atmospheric Reconnaissance and Research in Orbit (PISSARRO) (Goutam Chattapahyay/JPL) 7

8 Title Ultra Compact Short Wavelength Infrared imaging Spectrometer (UC-SWIRS) PI: Robert O. Green / Jet Propulsion Laboratory TRL = 6 Platform: Compatible with Venus Lander, Balloon, or Orbiter Key Capabilities: Spectral range: 0.4 to 5 microns full range or subset Spectral sampling: 10 nm adaptable to requirements Radiometric range: 0 to specific saturation Radiometric sampling: 16 bits Spatial swath: ~5 to 45 degrees adapted to requirements Spatial sampling: 0.1 to 1 milliradians adapted to requirements) Key Advantages over State of the Art: Collects measurements with full spectral and image content Multiple octaves of spectrum collected with single detector and instrument Nominal mass: 3kg function of exact requirements Nominal power: 3 W function of environment Onboard compression/analysis Contact Information: Name: Robert O. Green Institution: Jet Propulsion Laboratory Robert.O.Green@jpl.nasa.gov UC-SWIRS engineering model. UC-SWIRS can be configured for lander, Balloon or Orbiter science investigations. Example UC-SWIRS Lander image cube Example UC-SWIRS Orbiter image cube New Science Enabled: Spectroscopy from the visible through short wavelength infrared with image coverage A broad range of material composition and process investigations Specific science investigations are a function of the platform and refined requirements Planetary Exploration Science Technology Office (PESTO)

9 Venus: Trace Gas Measurements with an Eddy Flux Option PI: Scot Rafkin/Southwest Research Institute TRL = 6 Platform: Lander, Balloon, or Probe! Choose one, two or all three! Key Capabilities: Integrated acoustic anemometer and laser spectrometer for eddy flux measurements of momentum, energy and trace gases. Spectrometer available as stand alone instrument for key trace gas measurements (SO 2, OCS, H 2 SO 4, H 2 O, CO, H 2 S, HCL ) with necessary accuracy and sensitivity. Rapid measurement: > 1 Hz Modular subsystem design is easily adaptable to different platforms and even other planets. Key Advantages over State of the Art: Fast response to capture fine structures. Up to 8 unique channels; expansion possible. Robust against corrosion, high temp and press. Low Resource (<1 W, < 1 kg). Onboard data processing minimizes data volume. Solid state laser and optics, no moving parts. Can be integrated with acoustic anemometer for simultaneous wind and eddy flux measurements. Contact Information: Name: Scot Rafkin Institution: Southwest Research Institute (Boulder) rafkin.swri@gmail.com Laser I/F Box Integrated anemometer and spectrometer Control Electronic Box Figure Caption: Modular instrument design. Optical cell with patented mirror design is ~10 cm in length. Can be integrated on to an acoustic anemometer for eddy flux measurements. Integrated acoustic anemometer and laser spectrometer (with laser path shown by red line) undergoing field testing (inset, above). New Science Enabled: Rapid measurement of multiple trace gases to capture fine structure on descent or fast variations on a balloon or at the surface. Simultaneous measurement of key chemical species to assist in closure of chemical cycling. Addition of eddy flux provides dynamical source term for momentum, heat and mass. Planetary Exploration Science Technology Office (PESTO) Optical Cell (~10 cm)

10 Submillimeter-Wave Spectrometer Instrument for Venus Exploration PI: Goutam Chattopadhyay/Jet Propulsion Laboratory TRL = 5 Platform: Venus Orbiter Key Capabilities: A submillimeter-wave limb sounder providing unique data on the atmospheric physics and composition of Venus atmosphere. High-resolution submillimeter-wave spectrometer instrument allows sub-ppb sensitivity for trace species, direct temperature, pressure, wind measurements. High-TRL instrument matured through MatISSE investments. Flight heritage: based on proven technologies from SWAS, Herschel, EOS Aura, and Rosetta MIRO instrument. Key Advantages over State of the Art: MIRO was 19 Kg and needed 88 W DC of power. This instrument uses weighs less than 7 Kg and needs less than 12 W of DC power. Uses state-of-the-art CMOS all digital back-end spectrometers and low-power frequency synthesizer. Contact Information: Name: Goutam Chattopadhyay Institution: Jet Propulsion Laboratory goutam@jpl.nasa.gov Flip Mirror Calibration Load RF Front-End New Science Enabled: Synthesizer Digital Spectrometer Digital Spectrometer High-TRL low-mass and power (12W) highly-integrated submillimeter-wave spectrometer for Venus exploration. The entire instrument can fitin 2U form factor. Provide elemental and isotopic compositions of species in Venus atmosphere, especially the noble gases and nitrogen-, hydrogen-, carbon-, and sulfur-bearing species. Provide the knowledge of how the global atmospheric circulation patterns of Venus differ from those of Earth and Mars. Provide information related to the key processes, reactions, and chemical cycles controlling the chemistry of the middle, upper, and lower atmosphere of Venus. Determine how solar energy drives atmospheric circulation, cloud formation, and chemical cycles that define the current climate on terrestrial planets. Planetary Exploration Science Technology Office (PESTO)

11 Title: Venus Climate Sounder PI: M. Kenyon/JPL TRL = 5 Platform: Orbiter Mars Climate Sounder (MCS) Venus Climate Sounder (VCS) Key Capabilities: CRITICAL HERITAGE: Venus Climate Sounder (VCS) builds on Mars Climate Sounder (MCS) w/ simple mods to achieve half scale height limb profiling from low, polar, circular Venus orbit BETTER DESIGN: Keeps MCS excellent radiometric stability and accuracy but uses only one telescope (smaller/simpler) RELIABLE & CHEAP(ER): No cooler or active cooling of anything Key Advantages over State-of-the-Art: PERFECT PITCH: Use new large format thermopile array with 2x smaller pixel pitch to achieve FOV COVERS ALL WAVELENGTHS: Detectors measure from um with near perfect efficiency LONG STARES AT LIMB: Negligible lowfrequency (1/f) noise in detector-signal chain allow for long integration times for high signalto-noise Contact Information: Matt Kenyon JPL mkenyon@jpl.nasa.gov Figure: (Left) MCS has returned daily global maps of temperature, pressure, dust and ice from Mars, from the surface to 80km for more than 11 years. (Right) VCS incorporates all the design features of MCS for high accuracy radiometry, but utilizes a modern thermopile array that reduces the FOV by 2x and includes 10 spectral channels in a single telescope. New Science Enabled: Address Decadal Science: (i) How do the global atmospheric circulation patterns of Venus differ from those of Earth and Mars? (iii) What are the influences of clouds on radiative balances of planetary atmospheres, including cloud properties: microphysics, morphology, dynamics and coverage? Global structure of middle atmosphere mapped with half scale height (2-3 km) vertical resolution from the cloud tops to 110 km, both day and night. Global variation of temp, pres, aerosol opacity and water vapor over day/year Improved understanding of the structure and circulation of the middle atmosphere of Venus Planetary Exploration Science Technology Office (PESTO)